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Starlight Fleming-Maury-Cannon Classifications & Hertzsprung-Russell Diagram

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Starlight Fleming-Maury-Cannon Classifications & Hertzsprung-Russell Diagram STARLIGHT FLEMING-MAURY-CANNON CLASSIFICATIONS & HERTZSPRUNG-RUSSELL DIAGRAM IRINA RABEJA MEE DCSc CONTENT INTRODUCTION BRIGHTNESS OF STARS SPECTRUM OF LIGHT BEGINNING OF MODERN ASTRONOMY INTRODUCTION “The friendly gloss of stars on the night sky hides not only the Unknown but also the immense variety of the stars that often wander as double, triple and even quadruple, are either small as our Earth or big as our solar system, with an oscillating luminosity since they regularly expand and contract. And although the life of the stars is measured in billions years, they age also and ultimately die or simply cool down until their gloss is weaker and goes off or contrary collapse and explode in a powerful fireball. But still while the old pass new stars are born.” Our Earth is only a very small part of what we call the “universe” commonly defined as the totality of everything that exists. The word “universe” is derived from the Latin word universum, which connects uni (one) with versum (rolled/rotated), used in the sense everything rolled/rotated as one or everything combined into one. The universe was perceived by people from ancestral times as the sky with stars visible at night by their spot. The starlight is the only thing that comes from or is given by universe to us. But today only from the starlight the astronomers have knowledge about the chemical composition of the stars and other attributes like surface temperature, age, absolute magnitude, luminosity, diameter, mass, volume, density, distance from Earth, velocity, speed of rotation, magnetic field. And that happened by observing and analysing only two unmistakeable/distinctive properties of the stars: ▪ brightness (study originated in antiquity by Hipparchus) ▪ spectrum (study done first time by Joseph von Fraunhofer) They have opened the door to universe. BRIGHTNESS OF STARS Around the year 120 BC the Greek astronomers divided the stars visible to the naked eye into 6 classes function of their brightness B, from the brightest stars of class 1 to the faintest stars of class 6 at the limit of human visual perception. The brightness was measured in magnitude(s), class 1 having magnitude 1, class 2 having magnitude 2… class 6 with magnitude 6. Each class had twice the brightness of the following class, a total range of 6 magnitudes in logarithmic scale. Originated by Hipparchus, this method was popularized by Ptolemy in his Almagest, a second century ancient Greek mathematical and astronomical treatise on the complex motions of the stars and planetary paths, its geocentric model accepted as dogma for more than 12 hundred years until Copernicus. Norman Robert Pogson (1829-1891) formalized the system in 1856 year by defining a typical first class star (of magnitude 1) as a star that is 100 times brighter than a typical sixth class star (of magnitude 6), a magnitude 1 star being 2.512 times brighter than a magnitude 2 star, which is 2.512 times brighter than a magnitude 3 star and so on, where: 2.512 = 5√100 = Pogson’s Ratio The modern astronomy has kept in principle the same system, however is not limited to 6 magnitudes or only visible light, the scale has become enlarged (extended) to the extreme faint sky objects on one direction and on the other direction to the brightest heavenly bodies whose magnitudes are negative as Sirius (–1.4) full Moon (–12.74) or Sun (–26.74). The Hubble Space Telescope has located stars with brightness of magnitude +30 to +31 at visible wavelength and Keck telescopes have located similarly faint stars in infrared. However those magnitudes do not show the real light radiation of the star; they express a combination of the real spread of light of a star and its distance from Earth, for example a faint star would appear brighter at a shorter distance from Earth or the closest star to us, Sun, will appear a dot of light at enough farther distance. What is observed from Earth is the apparent brightness Bm measured in apparent magnitude(s) marked m, see FIG1. As measure for the real spread of light of a star, the astronomers defined the absolute brightness BM measured in absolute magnitude(s) marked M, see FIG 2. That is the brightness of the same star situated at a standard distance of 10 parsecs from Earth, examples: Sirius (1.4) or Sun (4.8). Parsec (pc) is a unit of length meaning parallax of one arc second. 1pc=31x1012 km=206,265 AU~3.26 light-years Parallax is the angular difference in the star apparent positions observed from opposite sides of Earth’s orbit. Knowing the distance D (in parsecs) between a star and Earth and the apparent brightness Bm of that star it is possible to calculate the absolute brightness BM of that star with the formula: BM = 5 + Bm – 5(log D) To express scientifically the amount of electromagnetic energy radiated per unit of time by star (the power output of a star) it is used the term luminosity marked L. Considering the luminosity of Sun as unit of measurement Lsun=1, the luminosity of any star can be obtained by knowing its absolute brightness BM with the formula: L = 10 –0.4 (BM – 4.8) Based on the Stefan-Boltzman law the luminosity of a star can be expressed as a function of its radius R and its surface temperature T: L = 4 π R2 σ T4 Higher the temperature and bigger the surface greater the energy flow in consequence the luminosity. For two stars of luminosity L1 and L2 their luminosity ratio is function of their radius square ratio and the fourth power of their temperature ratio: 2 4 2 4 L1 / L2 = 4 π σ R 1T 1 / 4 π σ R 2T 2 2 4 2 4 L1 / L2 = R 1T 1 / R 2T 2 Our Sun has a luminosity of 3.84x1026 W (Js-1) and a radius of 695 500 km. In astronomical calculations it is often more convenient to consider Sun as unit of measurement for stars by stating: Unit for luminosity of stars Lsun Unit for radius of stars Rsun Unit for mass of stars µsun Any other stars are compared with Sun. The radius R of a star can be evaluated when it is in the previous relation with Sun by knowing its temperature T and luminosity L: 2 2 R = (T sun/T ) √L Analysing the luminosity and the mass for different stars, was found that the luminosity of a star is bigger when its provision of energy is bigger meaning its mass is bigger. Resulted the relation between mass µ and luminosity L, mass-luminosity formula: L = µ3.5 In consequence the mass µ of a star can be obtained knowing the luminosity L of that star: µ = 3.5√L So, from the observed or apparent brightness of a star Bm it is possible to calculate for that star: ■ absolute brightness BM=5+Bm–5(log D) ■ luminosity L = 10–0.4(BM–4.78) 2 2 ■ radius R = (T sun / T )√L ■ mass µ = 3.5√L SPECTRUM OF LIGHT The light began to reveal its secrets in the year 1666 when the genial English mathematician and Nature scientist, Isaac Newton, directed a ray from Sun through a prism and saw that on the wall of his room appeared the colours of rainbow. To name the multicolour band that appeared like by magic on the wall of room, Newton took from Latin language the word spectrum meaning “ghost appearance” or “phantom”. The prism decomposed the light in a row of colours entering lightly one in another from red, through orange, yellow, green and blue to violet. Isaac Newton proved, what other thinkers agreed before, that the white light unifies in itself all the colours of the rainbow. The set of main colours in spectrum are shown in fig 3. In 1900 years researchers studied in laboratory the spectrum of the light coming from the flame of different glowing burning gases, found bright lines of different colours and called them spectral lines of the emissions spectrum see FIG 4. The researchers also found dark lines in the colours of spectra of Sun and other stars and called them the spectral lines of the absorptions spectrum, see FIG 5. The many dark lines in spectra have a chemical origin and their observations and analyses led to the discovery of the code of cosmic chemistry. The astronomers have developed a method to identify the chemical elements that generate the dark lines in spectrum by comparing carefully the spectrum of the star light with the spectrum of different burning gases light obtained in laboratory. The colours in spectrum are visible electromagnetic radiations with wavelengths 400nm – 700nm, see FIG 6. In 1900 year Max Planck (1858-1947), a German physicist, theorized that the electromagnetic radiation is emitted by a hot body in certain quantities, quanta. The light quanta are the photons. A spectral line is a bright line or a dark line in an otherwise uniform and continuous spectrum, resulting from an excess or a deficiency of photons in a narrow frequency range, compared with the nearby frequencies. RED ORANGE YELLOW GREEN AGVA BLUE INDIGO VIOLET 700-665 630 600 550 490 470 425 400 nm FIG 6 THE COLOURS OF STARLIGHT AND THEIR WAVELENGTHS The system of classification for stars based on the presence and strength of various types of absorption lines in their spectrum is called the spectral type. The large-angle telescopes of the astronomical observatories equipped with special prisms can take hundreds of star-spectrums simultaneously as photo images, see the photo with spectra of stars from the star cluster Hyades in FIG 7.
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